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We present a study of the Milky Way disk and halo magnetic field, determinedfrom observations of Faraday rotation measure (RM) towards 641 polarizedextragalactic radio sources in the Galactic longitude range 100-117 degs,within 30 degs of the Galactic plane. For |b| < 15 degs, we observe a symmetricRM distribution about the Galactic plane. This is consistent with a disk fieldin the Perseus arm of even parity across the Galactic mid-plane. In the range15<|b|<30 degs, we find median rotation measures of -15+/-4 rad/m^2 and -62+/-5rad/m^2 in the northern and southern Galactic hemispheres, respectively. If theRM distribution is a signature of the large-scale field parallel to theGalactic plane, this suggests that the halo magnetic field toward the outerGalaxy does not reverse direction across the mid-plane. The variation of RM asa function of Galactic latitude in this longitude range is such that RMs becomemore negative at larger |b|. This is consistent with an azimuthal magneticfield of strength 2 microGauss (7 microGauss) at a height 0.8-2 kpc above(below) the Galactic plane between the local and the Perseus spiral arm. Wepropose that the Milky Way could possess spiral-like halo magnetic fieldssimilar to those observed in M51.

New Constraints on the Galactic Halo Magnetic Field using Rotation Measures of Extragalactic Sources Towards the Outer Galaxy